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We report results from the first radiative particle-in-cell simulations ofstrong Alfvenic turbulence in plasmas of moderate optical depth. Thesimulations are performed in a local 3D periodic box and self-consistentlyfollow the evolution of radiation as it interacts with a turbulentelectron-positron plasma via Compton scattering. We focus on the conditionsexpected in magnetized coronae of accreting black holes and obtain an emissionspectrum consistent with the observed hard state of Cyg X-1. Most of theturbulence power is transferred directly to the photons via bulkComptonization, shaping the peak of the emission around 100 keV. The rest isreleased into nonthermal particles, which generate the MeV spectral tail. Themethod presented here shows promising potential for ab initio modeling ofvarious astrophysical sources and opens a window into a new regime of kineticplasma turbulence.

Radiative Particle-in-Cell Simulations of Turbulent Comptonization in Magnetized Black-Hole Coronae